Project acronym AEROSOL
Project Astrochemistry of old stars:direct probing of unique chemical laboratories
Researcher (PI) Leen Katrien Els Decin
Host Institution (HI) KATHOLIEKE UNIVERSITEIT LEUVEN
Call Details Consolidator Grant (CoG), PE9, ERC-2014-CoG
Summary The gas and dust in the interstellar medium (ISM) drive the chemical evolution of galaxies, the formation of stars and planets, and the synthesis of complex prebiotic molecules. The prime birth places for this interstellar material are the winds of evolved (super)giant stars. These winds are unique chemical laboratories, in which a large variety of gas and dust species radially expand away from the star.
Recent progress on the observations of these winds has been impressive thanks to Herschel and ALMA. The next challenge is to unravel the wealth of chemical information contained in these data. This is an ambitious task since (1) a plethora of physical and chemical processes interact in a complex way, (2) laboratory data to interpret these interactions are lacking, and (3) theoretical tools to analyse the data do not meet current needs.
To boost the knowledge of the physics and chemistry characterizing these winds, I propose a world-leading multi-disciplinary project combining (1) high-quality data, (2) novel theoretical wind models, and (3) targeted laboratory experiments. The aim is to pinpoint the dominant chemical pathways, unravel the transition from gas-phase to dust species, elucidate the role of clumps on the overall wind structure, and study the reciprocal effect between various dynamical and chemical phenomena.
Now is the right time for this ambitious project thanks to the availability of (1) high-quality multi-wavelength data, including ALMA and Herschel data of the PI, (2) supercomputers enabling a homogeneous analysis of the data using sophisticated theoretical wind models, and (3) novel laboratory equipment to measure the gas-phase reaction rates of key species.
This project will have far-reaching impact on (1) the field of evolved stars, (2) the understanding of the chemical lifecycle of the ISM, (3) chemical studies of dynamically more complex systems, such as exoplanets, protostars, supernovae etc., and (4) it will guide new instrument development.
Summary
The gas and dust in the interstellar medium (ISM) drive the chemical evolution of galaxies, the formation of stars and planets, and the synthesis of complex prebiotic molecules. The prime birth places for this interstellar material are the winds of evolved (super)giant stars. These winds are unique chemical laboratories, in which a large variety of gas and dust species radially expand away from the star.
Recent progress on the observations of these winds has been impressive thanks to Herschel and ALMA. The next challenge is to unravel the wealth of chemical information contained in these data. This is an ambitious task since (1) a plethora of physical and chemical processes interact in a complex way, (2) laboratory data to interpret these interactions are lacking, and (3) theoretical tools to analyse the data do not meet current needs.
To boost the knowledge of the physics and chemistry characterizing these winds, I propose a world-leading multi-disciplinary project combining (1) high-quality data, (2) novel theoretical wind models, and (3) targeted laboratory experiments. The aim is to pinpoint the dominant chemical pathways, unravel the transition from gas-phase to dust species, elucidate the role of clumps on the overall wind structure, and study the reciprocal effect between various dynamical and chemical phenomena.
Now is the right time for this ambitious project thanks to the availability of (1) high-quality multi-wavelength data, including ALMA and Herschel data of the PI, (2) supercomputers enabling a homogeneous analysis of the data using sophisticated theoretical wind models, and (3) novel laboratory equipment to measure the gas-phase reaction rates of key species.
This project will have far-reaching impact on (1) the field of evolved stars, (2) the understanding of the chemical lifecycle of the ISM, (3) chemical studies of dynamically more complex systems, such as exoplanets, protostars, supernovae etc., and (4) it will guide new instrument development.
Max ERC Funding
2 605 897 €
Duration
Start date: 2016-01-01, End date: 2020-12-31
Project acronym AIDA
Project An Illumination of the Dark Ages: modeling reionization and interpreting observations
Researcher (PI) Andrei Albert Mesinger
Host Institution (HI) SCUOLA NORMALE SUPERIORE
Call Details Starting Grant (StG), PE9, ERC-2014-STG
Summary "Understanding the dawn of the first galaxies and how their light permeated the early Universe is at the very frontier of modern astrophysical cosmology. Generous resources, including ambitions observational programs, are being devoted to studying these epochs of Cosmic Dawn (CD) and Reionization (EoR). In order to interpret these observations, we propose to build on our widely-used, semi-numeric simulation tool, 21cmFAST, and apply it to observations. Using sub-grid, semi-analytic models, we will incorporate additional physical processes governing the evolution of sources and sinks of ionizing photons. The resulting state-of-the-art simulations will be well poised to interpret topical observations of quasar spectra and the cosmic 21cm signal. They would be both physically-motivated and fast, allowing us to rapidly explore astrophysical parameter space. We will statistically quantify the resulting degeneracies and constraints, providing a robust answer to the question, ""What can we learn from EoR/CD observations?"" As an end goal, these investigations will help us understand when the first generations of galaxies formed, how they drove the EoR, and what are the associated large-scale observational signatures."
Summary
"Understanding the dawn of the first galaxies and how their light permeated the early Universe is at the very frontier of modern astrophysical cosmology. Generous resources, including ambitions observational programs, are being devoted to studying these epochs of Cosmic Dawn (CD) and Reionization (EoR). In order to interpret these observations, we propose to build on our widely-used, semi-numeric simulation tool, 21cmFAST, and apply it to observations. Using sub-grid, semi-analytic models, we will incorporate additional physical processes governing the evolution of sources and sinks of ionizing photons. The resulting state-of-the-art simulations will be well poised to interpret topical observations of quasar spectra and the cosmic 21cm signal. They would be both physically-motivated and fast, allowing us to rapidly explore astrophysical parameter space. We will statistically quantify the resulting degeneracies and constraints, providing a robust answer to the question, ""What can we learn from EoR/CD observations?"" As an end goal, these investigations will help us understand when the first generations of galaxies formed, how they drove the EoR, and what are the associated large-scale observational signatures."
Max ERC Funding
1 468 750 €
Duration
Start date: 2015-05-01, End date: 2021-01-31
Project acronym B Massive
Project Binary massive black hole astrophysics
Researcher (PI) Alberto SESANA
Host Institution (HI) UNIVERSITA' DEGLI STUDI DI MILANO-BICOCCA
Call Details Consolidator Grant (CoG), PE9, ERC-2018-COG
Summary Massive black hole binaries (MBHBs) are the most extreme, fascinating yet elusive astrophysical objects in the Universe. Establishing observationally their existence will be a milestone for contemporary astronomy, providing a fundamental missing piece in the puzzle of galaxy formation, piercing through the (hydro)dynamical physical processes shaping dense galactic nuclei from parsec scales down to the event horizon, and probing gravity in extreme conditions.
We can both see and listen to MBHBs. Remarkably, besides arguably being among the brightest variable objects shining in the Cosmos, MBHBs are also the loudest gravitational wave (GW) sources in the Universe. As such, we shall take advantage of both the type of messengers – photons and gravitons – they are sending to us, which can now be probed by all-sky time-domain surveys and radio pulsar timing arrays (PTAs) respectively.
B MASSIVE leverages on a unique comprehensive approach combining theoretical astrophysics, radio and gravitational-wave astronomy and time-domain surveys, with state of the art data analysis techniques to: i) observationally prove the existence of MBHBs, ii) understand and constrain their astrophysics and dynamics, iii) enable and bring closer in time the direct detection of GWs with PTA.
As European PTA (EPTA) executive committee member and former I
International PTA (IPTA) chair, I am a driving force in the development of pulsar timing science world-wide, and the project will build on the profound knowledge, broad vision and wide collaboration network that established me as a world leader in the field of MBHB and GW astrophysics. B MASSIVE is extremely timely; a pulsar timing data set of unprecedented quality is being assembled by EPTA/IPTA, and Time-Domain astronomy surveys are at their dawn. In the long term, B MASSIVE will be a fundamental milestone establishing European leadership in the cutting-edge field of MBHB astrophysics in the era of LSST, SKA and LISA.
Summary
Massive black hole binaries (MBHBs) are the most extreme, fascinating yet elusive astrophysical objects in the Universe. Establishing observationally their existence will be a milestone for contemporary astronomy, providing a fundamental missing piece in the puzzle of galaxy formation, piercing through the (hydro)dynamical physical processes shaping dense galactic nuclei from parsec scales down to the event horizon, and probing gravity in extreme conditions.
We can both see and listen to MBHBs. Remarkably, besides arguably being among the brightest variable objects shining in the Cosmos, MBHBs are also the loudest gravitational wave (GW) sources in the Universe. As such, we shall take advantage of both the type of messengers – photons and gravitons – they are sending to us, which can now be probed by all-sky time-domain surveys and radio pulsar timing arrays (PTAs) respectively.
B MASSIVE leverages on a unique comprehensive approach combining theoretical astrophysics, radio and gravitational-wave astronomy and time-domain surveys, with state of the art data analysis techniques to: i) observationally prove the existence of MBHBs, ii) understand and constrain their astrophysics and dynamics, iii) enable and bring closer in time the direct detection of GWs with PTA.
As European PTA (EPTA) executive committee member and former I
International PTA (IPTA) chair, I am a driving force in the development of pulsar timing science world-wide, and the project will build on the profound knowledge, broad vision and wide collaboration network that established me as a world leader in the field of MBHB and GW astrophysics. B MASSIVE is extremely timely; a pulsar timing data set of unprecedented quality is being assembled by EPTA/IPTA, and Time-Domain astronomy surveys are at their dawn. In the long term, B MASSIVE will be a fundamental milestone establishing European leadership in the cutting-edge field of MBHB astrophysics in the era of LSST, SKA and LISA.
Max ERC Funding
1 532 750 €
Duration
Start date: 2019-09-01, End date: 2024-08-31
Project acronym BOSS-WAVES
Project Back-reaction Of Solar plaSma to WAVES
Researcher (PI) Tom VAN DOORSSELAERE
Host Institution (HI) KATHOLIEKE UNIVERSITEIT LEUVEN
Call Details Consolidator Grant (CoG), PE9, ERC-2016-COG
Summary "The solar coronal heating problem is a long-standing astrophysical problem. The slow DC (reconnection) heating models are well developed in detailed 3D numerical simulations. The fast AC (wave) heating mechanisms have traditionally been neglected since there were no wave observations.
Since 2007, we know that the solar atmosphere is filled with transverse waves, but still we have no adequate models (except for my own 1D analytical models) for their dissipation and plasma heating by these waves. We urgently need to know the contribution of these waves to the coronal heating problem.
In BOSS-WAVES, I will innovate the AC wave heating models by utilising novel 3D numerical simulations of propagating transverse waves. From previous results in my team, I know that the inclusion of the back-reaction of the solar plasma is crucial in understanding the energy dissipation: the wave heating leads to chromospheric evaporation and plasma mixing (by the Kelvin-Helmholtz instability).
BOSS-WAVES will bring the AC heating models to the same level of state-of-the-art DC heating models.
The high-risk, high-gain goals are (1) to create a coronal loop heated by waves, starting from an "empty" corona, by evaporating chromospheric material, and (2) to pioneer models for whole active regions heated by transverse waves."
Summary
"The solar coronal heating problem is a long-standing astrophysical problem. The slow DC (reconnection) heating models are well developed in detailed 3D numerical simulations. The fast AC (wave) heating mechanisms have traditionally been neglected since there were no wave observations.
Since 2007, we know that the solar atmosphere is filled with transverse waves, but still we have no adequate models (except for my own 1D analytical models) for their dissipation and plasma heating by these waves. We urgently need to know the contribution of these waves to the coronal heating problem.
In BOSS-WAVES, I will innovate the AC wave heating models by utilising novel 3D numerical simulations of propagating transverse waves. From previous results in my team, I know that the inclusion of the back-reaction of the solar plasma is crucial in understanding the energy dissipation: the wave heating leads to chromospheric evaporation and plasma mixing (by the Kelvin-Helmholtz instability).
BOSS-WAVES will bring the AC heating models to the same level of state-of-the-art DC heating models.
The high-risk, high-gain goals are (1) to create a coronal loop heated by waves, starting from an "empty" corona, by evaporating chromospheric material, and (2) to pioneer models for whole active regions heated by transverse waves."
Max ERC Funding
1 991 960 €
Duration
Start date: 2017-10-01, End date: 2022-09-30
Project acronym ClustersXCosmo
Project Fundamental physics, Cosmology and Astrophysics: Galaxy Clusters at the Cross-roads
Researcher (PI) Alexandro SARO
Host Institution (HI) UNIVERSITA DEGLI STUDI DI TRIESTE
Call Details Starting Grant (StG), PE9, ERC-2016-STG
Summary The ClustersXCosmo ERC Starting Grant proposal has the goal of investigating the role of Galaxy Clusters as a cosmological probe and of exploiting the strong synergies between observational cosmology, galaxy formation and fundamental physics related to the tracers of the extreme peaks in the matter density field. In the last decade, astronomical data-sets have started to be widely and quantitatively used by the scientific community to address important physical questions such as: the nature of the dark matter and dark energy components and their evolution; the physical properties of the baryonic matter; the variation of fundamental constants over cosmic time; the sum of neutrino masses; the interplay between the galaxy population and the intergalactic medium; the nature of gravity over megaparsec scales and over cosmic times; the temperature evolution of the Universe. Most of these results are based on well-established geometrical cosmological probes (e.g., galaxies, supernovae, cosmic microwave background). Galaxy clusters provide a complementary and necessary approach, as their distribution as a function of time and observables is sensitive to both the geometrical and the dynamical evolution of the Universe, driven by the growth of structures. Among different cluster surveys, Sunyaev Zel'Dovich effect (SZE) detected catalogs have registered the most dramatic improvement over the last ~5 years, yielding samples extending up to the earliest times these systems appeared. This proposal aims at using a combination of the best available SZE cluster surveys and to interpret them by means of state-of-the-art computational facilities in order to firmly establish the yet controversial role of Galaxy Clusters as a probe for cosmology, fundamental physics and astrophysics. The timely convergence of current and next generation multi-wavelength surveys (DES/SPT/Planck/eRosita/Euclid) will be important to establish the role of Galaxy Clusters as a cosmological tool.
Summary
The ClustersXCosmo ERC Starting Grant proposal has the goal of investigating the role of Galaxy Clusters as a cosmological probe and of exploiting the strong synergies between observational cosmology, galaxy formation and fundamental physics related to the tracers of the extreme peaks in the matter density field. In the last decade, astronomical data-sets have started to be widely and quantitatively used by the scientific community to address important physical questions such as: the nature of the dark matter and dark energy components and their evolution; the physical properties of the baryonic matter; the variation of fundamental constants over cosmic time; the sum of neutrino masses; the interplay between the galaxy population and the intergalactic medium; the nature of gravity over megaparsec scales and over cosmic times; the temperature evolution of the Universe. Most of these results are based on well-established geometrical cosmological probes (e.g., galaxies, supernovae, cosmic microwave background). Galaxy clusters provide a complementary and necessary approach, as their distribution as a function of time and observables is sensitive to both the geometrical and the dynamical evolution of the Universe, driven by the growth of structures. Among different cluster surveys, Sunyaev Zel'Dovich effect (SZE) detected catalogs have registered the most dramatic improvement over the last ~5 years, yielding samples extending up to the earliest times these systems appeared. This proposal aims at using a combination of the best available SZE cluster surveys and to interpret them by means of state-of-the-art computational facilities in order to firmly establish the yet controversial role of Galaxy Clusters as a probe for cosmology, fundamental physics and astrophysics. The timely convergence of current and next generation multi-wavelength surveys (DES/SPT/Planck/eRosita/Euclid) will be important to establish the role of Galaxy Clusters as a cosmological tool.
Max ERC Funding
1 230 403 €
Duration
Start date: 2017-09-01, End date: 2022-08-31
Project acronym COSMIC-LAB
Project Star clusters as cosmic laboratories for Astrophysics, Dynamics and Fundamental Physics
Researcher (PI) Francesco Ferraro
Host Institution (HI) ALMA MATER STUDIORUM - UNIVERSITA DI BOLOGNA
Call Details Advanced Grant (AdG), PE9, ERC-2010-AdG_20100224
Summary "Galactic Globular Clusters (GCs) are the most populous, old and dense stellar systems in the Galaxy. Their study addresses fundamental astrophysical questions, ranging from the Galaxy formation, to stellar evolution and dynamics. With Cosmic-Lab we intend to use these natural laboratories to perform three original experiments which will have a major impact on several areas of modern Physics and Astrophysics. To this aim we will adopt as test particles three classes of ""exotica"" (namely blue stragglers - BSS, millisecond pulsars -MSPs, and intermediate-mass black holes -IMBHs):
Exp 1 - ""Toward the definition of a dynamical clock for stellar systems"". By exploiting our exceptional multi-wavelength database, we propose to use the observed properties of BSS for defining an innovative tool to measure the degree of dynamical evolution of collisional stellar systems.
Exp 2 - ""Hunting for the most massive neutron stars (NSs): probing the equation of state of matter at nuclear densities"" - We propose to search for the companion stars to binary MSPs in a selected sample of GCs thus to exploit the unique opportunity offered by these systems to measure the NS masses. This will finally allow us to determine the upper limit to the NS mass and tightly constrain the equation of state of matter at the nuclear equilibrium density.
Exp 3 - ""IMBHs: the missing link in the formation of cosmic structures"" - We propose to use a set of non-conventional data-analysis procedures developed by our group in order to unveil IMBHs at the center of GCs. Proving the existence of these objects is crucial for understanding the formation of super-massive BHs, which are observed at the centre of all massive galaxies at any redshift, with a major impact on the comprehension of the formation and evolution of cosmic structures."
Summary
"Galactic Globular Clusters (GCs) are the most populous, old and dense stellar systems in the Galaxy. Their study addresses fundamental astrophysical questions, ranging from the Galaxy formation, to stellar evolution and dynamics. With Cosmic-Lab we intend to use these natural laboratories to perform three original experiments which will have a major impact on several areas of modern Physics and Astrophysics. To this aim we will adopt as test particles three classes of ""exotica"" (namely blue stragglers - BSS, millisecond pulsars -MSPs, and intermediate-mass black holes -IMBHs):
Exp 1 - ""Toward the definition of a dynamical clock for stellar systems"". By exploiting our exceptional multi-wavelength database, we propose to use the observed properties of BSS for defining an innovative tool to measure the degree of dynamical evolution of collisional stellar systems.
Exp 2 - ""Hunting for the most massive neutron stars (NSs): probing the equation of state of matter at nuclear densities"" - We propose to search for the companion stars to binary MSPs in a selected sample of GCs thus to exploit the unique opportunity offered by these systems to measure the NS masses. This will finally allow us to determine the upper limit to the NS mass and tightly constrain the equation of state of matter at the nuclear equilibrium density.
Exp 3 - ""IMBHs: the missing link in the formation of cosmic structures"" - We propose to use a set of non-conventional data-analysis procedures developed by our group in order to unveil IMBHs at the center of GCs. Proving the existence of these objects is crucial for understanding the formation of super-massive BHs, which are observed at the centre of all massive galaxies at any redshift, with a major impact on the comprehension of the formation and evolution of cosmic structures."
Max ERC Funding
1 880 000 €
Duration
Start date: 2011-05-01, End date: 2016-04-30
Project acronym COSMOIGM
Project The Intergalactic Medium as a Cosmological Tool
Researcher (PI) Matteo Viel
Host Institution (HI) ISTITUTO NAZIONALE DI ASTROFISICA
Call Details Starting Grant (StG), PE9, ERC-2010-StG_20091028
Summary The cosmoIGM proposal aims at investigating the role of the Intergalactic Medium (IGM) as a cosmological probe and at exploiting the many IGM-related sinergies between observational cosmology, galaxy formation and fundamental physics. The IGM is a unique cosmological observable as it probes 3/4 of the present age of the universe, it contains up to 80% of the baryons and is sensitive to scales that are not measured by other data. In the last decade, astronomical data sets have started to be widely used by the scientific community to address important physical issues such as: the nature of the dark matter and dark energy components and their evolution; the physical properties of the baryonic matter; variation of fundamental constants; feedback processes by galaxies, etc. For example, results obtained from astronomical data are nowadays comparable to those obtained by ground based physics laboratories (e.g. neutrino masses). This proposal will rely on observations of the IGM at high and low redshift and will interpret them by means of state-of-the-art computational facilities in order to firmly establish the (yet controversial) role of the IGM as a probe for cosmology and fundamental physics. Moreover, we aim at exploring the galaxy-IGM interplay at a crucial stage of the cosmic history when the universe was few Gyrs old and star forming galaxies were strongly affecting the dynamical, thermal and chemical properties of the IGM. The hosting institution, Trieste Observatory, and the Trieste Area (ICTP, SISSA and Trieste University) have a long-standing expertise on the topics above. We foresee that the present interdisciplinary proposal will have a strong scientific impact and will help the P.I. to consolidate its independence and to create his first research team.
Summary
The cosmoIGM proposal aims at investigating the role of the Intergalactic Medium (IGM) as a cosmological probe and at exploiting the many IGM-related sinergies between observational cosmology, galaxy formation and fundamental physics. The IGM is a unique cosmological observable as it probes 3/4 of the present age of the universe, it contains up to 80% of the baryons and is sensitive to scales that are not measured by other data. In the last decade, astronomical data sets have started to be widely used by the scientific community to address important physical issues such as: the nature of the dark matter and dark energy components and their evolution; the physical properties of the baryonic matter; variation of fundamental constants; feedback processes by galaxies, etc. For example, results obtained from astronomical data are nowadays comparable to those obtained by ground based physics laboratories (e.g. neutrino masses). This proposal will rely on observations of the IGM at high and low redshift and will interpret them by means of state-of-the-art computational facilities in order to firmly establish the (yet controversial) role of the IGM as a probe for cosmology and fundamental physics. Moreover, we aim at exploring the galaxy-IGM interplay at a crucial stage of the cosmic history when the universe was few Gyrs old and star forming galaxies were strongly affecting the dynamical, thermal and chemical properties of the IGM. The hosting institution, Trieste Observatory, and the Trieste Area (ICTP, SISSA and Trieste University) have a long-standing expertise on the topics above. We foresee that the present interdisciplinary proposal will have a strong scientific impact and will help the P.I. to consolidate its independence and to create his first research team.
Max ERC Funding
891 400 €
Duration
Start date: 2010-12-01, End date: 2016-11-30
Project acronym DARKLIGHT
Project ILLUMINATING DARK ENERGY WITH THE NEXT GENERATION OF COSMOLOGICAL REDSHIFT SURVEYS
Researcher (PI) Luigi Guzzo
Host Institution (HI) UNIVERSITA DEGLI STUDI DI MILANO
Call Details Advanced Grant (AdG), PE9, ERC-2011-ADG_20110209
Summary Galaxy redshift surveys have been central in establishing the current successful cosmological model. Reconstructing the large-scale distribution of galaxies in space and time, they provide us with a unique probe of the basic constituents of the Universe, their evolution and the background fundamental physics. A new generation of even larger surveys is planned for the starting decade, with the aim of solving the remaining mysteries of the standard model using high-precision measurements of galaxy clustering. These entail the nature of the “dark sector” and in particular the origin of the accelerated cosmic expansion. While data accumulation already started, the needed analysis capabilities to reach the required percent levels in both accuracy and precision are not ready yet.
I propose to establish a focused research group to develop these tools and optimally analyze the new data, while being directly involved in their collection. New techniques as redshift-space distortions and well-known but still debated probes as galaxy clusters will be refined to a new level. They will be combined with more standard methods as baryonic acoustic oscillations and external data as CMB anisotropies. Performances will be validated on mock samples from large numerical simulations and then applied to state-of-the-art data with enhanced control over systematic errors to obtain the best achievable measurements.
These new capabilities will be decisive in enabling ongoing and future surveys to tackle the key open problems in cosmology: What is the nature of dark energy? Is it produced by an evolving scalar field? Or does it rather require a modification of the laws of gravity? How does it relate to dark matter? What is the role of neutrinos? The answer to these questions may well revolutionize our view of physics.
Summary
Galaxy redshift surveys have been central in establishing the current successful cosmological model. Reconstructing the large-scale distribution of galaxies in space and time, they provide us with a unique probe of the basic constituents of the Universe, their evolution and the background fundamental physics. A new generation of even larger surveys is planned for the starting decade, with the aim of solving the remaining mysteries of the standard model using high-precision measurements of galaxy clustering. These entail the nature of the “dark sector” and in particular the origin of the accelerated cosmic expansion. While data accumulation already started, the needed analysis capabilities to reach the required percent levels in both accuracy and precision are not ready yet.
I propose to establish a focused research group to develop these tools and optimally analyze the new data, while being directly involved in their collection. New techniques as redshift-space distortions and well-known but still debated probes as galaxy clusters will be refined to a new level. They will be combined with more standard methods as baryonic acoustic oscillations and external data as CMB anisotropies. Performances will be validated on mock samples from large numerical simulations and then applied to state-of-the-art data with enhanced control over systematic errors to obtain the best achievable measurements.
These new capabilities will be decisive in enabling ongoing and future surveys to tackle the key open problems in cosmology: What is the nature of dark energy? Is it produced by an evolving scalar field? Or does it rather require a modification of the laws of gravity? How does it relate to dark matter? What is the role of neutrinos? The answer to these questions may well revolutionize our view of physics.
Max ERC Funding
1 723 600 €
Duration
Start date: 2012-05-01, End date: 2017-10-31
Project acronym DEMOBLACK
Project Demography of black hole binaries in the era of gravitational wave astronomy
Researcher (PI) Michela MAPELLI
Host Institution (HI) UNIVERSITA DEGLI STUDI DI PADOVA
Call Details Consolidator Grant (CoG), PE9, ERC-2017-COG
Summary The first direct detection of gravitational waves demonstrated that double black hole (BH) binaries exist, and can host surprisingly massive objects (> 20 solar masses). Most theoretical models do not predict the existence of such massive BHs, and the formation channels of BH binaries are essentially unconstrained. Dynamically formed BH binaries are the most elusive ones: current models either neglect them or study them in idealized systems. With DEMOBLACK, I will draw the first satisfactory picture of BH binary demography, by modeling realistic BH dynamics in a well-motivated cosmological context. I propose a novel approach for the study of BH dynamics: I will simulate the formation of BH binaries in star clusters self-consistently, starting from the hydrodynamics of the parent molecular cloud and accounting for the impact of stellar evolution, feedback, and dynamics on BH binaries. The key tool of DEMOBLACK is SEVN, my new population-synthesis code. With SEVN, I predicted the formation of massive BHs from metal-poor stars, before the first direct detection of gravitational waves. I will interface SEVN with a hydrodynamical code and with an N-body code, to study the formation of BH binaries self-consistently. I will then model the history of BH binaries across cosmic time, accounting for the evolution of metallicity. This novel approach is decisive to break degeneracies between dynamically formed and primordial BH binaries, and to make predictions for future observations by ground-based and space-borne gravitational wave interferometers.
Summary
The first direct detection of gravitational waves demonstrated that double black hole (BH) binaries exist, and can host surprisingly massive objects (> 20 solar masses). Most theoretical models do not predict the existence of such massive BHs, and the formation channels of BH binaries are essentially unconstrained. Dynamically formed BH binaries are the most elusive ones: current models either neglect them or study them in idealized systems. With DEMOBLACK, I will draw the first satisfactory picture of BH binary demography, by modeling realistic BH dynamics in a well-motivated cosmological context. I propose a novel approach for the study of BH dynamics: I will simulate the formation of BH binaries in star clusters self-consistently, starting from the hydrodynamics of the parent molecular cloud and accounting for the impact of stellar evolution, feedback, and dynamics on BH binaries. The key tool of DEMOBLACK is SEVN, my new population-synthesis code. With SEVN, I predicted the formation of massive BHs from metal-poor stars, before the first direct detection of gravitational waves. I will interface SEVN with a hydrodynamical code and with an N-body code, to study the formation of BH binaries self-consistently. I will then model the history of BH binaries across cosmic time, accounting for the evolution of metallicity. This novel approach is decisive to break degeneracies between dynamically formed and primordial BH binaries, and to make predictions for future observations by ground-based and space-borne gravitational wave interferometers.
Max ERC Funding
1 994 764 €
Duration
Start date: 2018-11-01, End date: 2023-10-31
Project acronym DRANOEL
Project Deciphering RAdio NOn-thermal Emission on the Largest scales
Researcher (PI) Annalisa BONAFEDE
Host Institution (HI) ALMA MATER STUDIORUM - UNIVERSITA DI BOLOGNA
Call Details Starting Grant (StG), PE9, ERC-2016-STG
Summary This proposal aims to understand the origin of the radio emission detected in the most massive objects in our Universe: galaxy clusters.
The extreme physical conditions in the intra-cluster medium of galaxy clusters are beyond anything achievable in any laboratory on Earth. The space in between the galaxies is filled with an extremely hot and diluted gas that hosts the largest-scale magnetic fields known so far. A big challenge of modern astrophysics is understanding the origin of radio emission spread over huge swathes in some clusters. This emission is a mystery because it requires relativistic electrons moving around magnetic field lines, but both the origin of the magnetic fields and of the electrons are unknown. Absolutely fundamental to the understanding of the radio emission are a detailed knowledge of the magnetic fields and of the energy spectrum of the emitting particles.
We are stepping into a new era of observational astronomy, in which surveys will be conducted rather than single pointed observations. This survey era is changing our approach to observational data. It enables to perform all-sky studies but calls for numerical and technological efforts for the data handling.
Taking advantage of the advent of new radio and X-ray facilities, such as LOFAR, the JVLA, ASKAP, and eROSITA, this project wants to understand the origin of the radio emission, its evolution and its connections with the cluster dynamics.
We have today the unprecedented opportunity to discover the physical processes at work in these unique environments, that link the micro-physical processes at work in galaxy clusters with the clusters' macro-physics. The proposed study will address fundamental questions not restricted to the physics of galaxy clusters but having impact on several inter-connected physical disciplines, such as cosmology, astro-particle physics and plasma physics.
Summary
This proposal aims to understand the origin of the radio emission detected in the most massive objects in our Universe: galaxy clusters.
The extreme physical conditions in the intra-cluster medium of galaxy clusters are beyond anything achievable in any laboratory on Earth. The space in between the galaxies is filled with an extremely hot and diluted gas that hosts the largest-scale magnetic fields known so far. A big challenge of modern astrophysics is understanding the origin of radio emission spread over huge swathes in some clusters. This emission is a mystery because it requires relativistic electrons moving around magnetic field lines, but both the origin of the magnetic fields and of the electrons are unknown. Absolutely fundamental to the understanding of the radio emission are a detailed knowledge of the magnetic fields and of the energy spectrum of the emitting particles.
We are stepping into a new era of observational astronomy, in which surveys will be conducted rather than single pointed observations. This survey era is changing our approach to observational data. It enables to perform all-sky studies but calls for numerical and technological efforts for the data handling.
Taking advantage of the advent of new radio and X-ray facilities, such as LOFAR, the JVLA, ASKAP, and eROSITA, this project wants to understand the origin of the radio emission, its evolution and its connections with the cluster dynamics.
We have today the unprecedented opportunity to discover the physical processes at work in these unique environments, that link the micro-physical processes at work in galaxy clusters with the clusters' macro-physics. The proposed study will address fundamental questions not restricted to the physics of galaxy clusters but having impact on several inter-connected physical disciplines, such as cosmology, astro-particle physics and plasma physics.
Max ERC Funding
1 496 250 €
Duration
Start date: 2017-09-01, End date: 2022-08-31
